Unfortunately, no planet transits were detected around stars in the M37 cluster, but an unrelated field star shows signs that it may have a Jupiter-radius planet in a 0.77 day orbit (an "extremely hot Jupiter" or to use the term that the SWEEPS survey used for planets in this period range, an ultra-short-period-planet). Because the star is faint, getting an RV confirmation will be tricky.

Modelling simulations by Wilner's team (including www.harvard.edu/hco/astro/people/homepages/holman.html" target="_blank" rel="nofollow">Matt Holman, www.harvard.edu/hco/astro/people/homepages/ho.html" target="_blank" rel="nofollow">Paul Ho, and Marc Kuchner) suggested that the semimajor axis of the planet's orbit may center around 30 AUs -- at Neptune's orbital distance in the Solar System. The simulations also indicated that the planet must be smaller than 30 times Jupiter's mass. A larger planetary mass would cause the observed dust clumps to overlap by destroying and the hypothesized orbital resonances

Then the Neptune-like planet model upcame and the "Vegan dwarf" were not discussed anymore.

Other simulations by Nick N. Gorkavyi and Tanya A. Taidakova (Schafer Corporation) of an observed dust disk ring arc at 95 AUs also suggested that there may be a sub-Jovian planet between 90 to 100 AUs out from Vega. The simulations indicated that one (or more) very massive planet within 50 to 60 AUs may have destroyed the inner circumstellar dust disk by gravitational scattering (Abstract for 2002 AAS session 86.07).

There is also an animation (Vega b looks quite eccentric too; e=0.6):

Assuming the planet laying at 30 AUs and e=0.6, we should have an object swinging between 12 AUs and 48 AUs (apastron). Moreover if the habitable zone lies at 7 AUs, such object would lay in system's water zone at periastron and beyond the snowline at apastron.

Context: Recent modeling based on unresolved infrared observations of the spectral energy distribution (SED) of GM Aurigae suggests that the inner disk of this single TTauri star is truncated at an inner radius of 25 AU. Aims: We attempt to find evidence of this inner hole in the gas distribution, using spectroscopy with high angular resolution. Methods: Using the IRAM array, we obtained high angular resolution ( 1.5”) observations with a high S/N per channel of the 13CO J=2{-}1 and C18O J=2{-}1 and of the 13CO J=1{-}0 lines. A standard parametric disk model is used to fit the line data in the Fourier-plane and to derive the CO disk properties. Our measurement is based on a detailed analysis of the spectroscopic profile from the CO disk rotating in Keplerian velocity. The millimeter continuum, tracing the dust, is also analyzed. Results: We detect an inner cavity of radius 19 ± 4 AU at the 4.5σ level. The hole manifests itself by a lack of emission beyond the (projected) Keplerian speed at the inner radius. We also constrain the temperature gradient in the disk. Conclusions: Our data reveal the existence of an inner hole in GM Aur gas disk. Its origin remains unclear, but can be linked to planet formation or to a low mass stellar companion orbiting close to the central star ( 5-15 AU). The frequent finding of inner cavities suggests that either binarity is the most common scenario of star formation in Taurus or that giant planet formation starts early

Probably the cavities observed in GM Aur's disk may be produced by two planets. A 5 Mj object at 8.5 AUs and a 5-10 Mj (probably 7 Mj) within 15 AUs.

We present the initial results of the analysis of the precise radial velocities of the relatively little-studied star delta Sagittarii, K2.5 IIIa, HR 6859. The data were obtained at the Canada-France-Hawaii Telescope using the hydrogen fluoride absorption cell technique. The periodogram shows significant peaks at 2.8 days (K=104 m s(-1) ), 63 days (K=85 m s(-1) ), and 295 days (K=72 m s(-1) ). Because of our limited data the true period cannot be distinguished from these possibilities due to aliasing. This giant is an interesting example of a star having a radial velocity periodicity which may be attributed to intrinsic variability, rotational modulation, or the presence of a low M_2 sin i companion (see A. Walker et al., this conference). More observations are urgently required to determine the true period and to discover the underlying origin for this star's radial velocity variability.

As we're talking about K giants, does anybody have a reference about the couple of brown dwarfs orbiting the bright K giant Iota Aurigae? Those were mentioned in a conference, I guess, has there been any update or paper about?

Using these values, I obtain a mass of the star 6.7 solar masses (this assumes that the radius and the gravity determination are measuring the same bit of the star of course). The distances of the two companions from the star would then be 3 AU and 5 AU. For comparison, the stellar radius is 0.53 AU. The planets will therefore be extremely hot!

Apart from the curious name of the author *LOL*, there is a possible evidence that secondary component of a hot white dwarf may be a Jupiter-mass (and sized) Jovian planet rather an usual M-dwarf. Orbital period spanning between 0.5-5 days. If true, this object would be 550 K hot.

1) Amongst possible explanations for Wolf 359's flare activity, a planetary companion may not be ruled out at all. Such an object would yield 20% of Jupiter's mass (0.2 Mj) and be located at 0.015 AUs from host star. If true, that would be the closest "Hot Jupiter" to our Sun.

... We note that Cumming et al. (2008, their fig. 5) have shown that in the Keck Planet search program a group of very massive candidates (M sin i >~ 20 M_J) at periods >~ 2000 d (a >~ 3 AU) exists which have not yet been announced.

The structure, formation and fate of hot Jupiter exoplanets is governed by the properties of their atmospheres. There is an urgent need for for strong observational constraints to guide the development of model atmospheres for hot Jupiters. WASP-17b is a newly discovered transiting hot Jupiter exoplanet. It has the lowest density of any transiting hot Jupiter discovered to-date. The host star, WASP-17, is a bright (VD11.6) F6V star. This combination of factors make WASP-17 a key object for testing the current paradigm in which hot pM class planets have stratospheres and cooler pL class planets do not. We will use Spitzer to observe the secondary eclipse of the planet by its host star at 3.6um and 4.5um, and use these data to measure the brightness temperature at these wavelenghs. In the current paradigm, this pM class planet should show evidence of a stratosphere from the ratio of the brightness temperatures at these wavelengths. We will also use transmission spectroscopy to determine independently whether WASP-17b has a stratoshere. VLT time to obtain the required spectroscopy has already been approved. WASP-17 is currently the only pM class planet apart from HD209458 for which the results from the two methods can be compared. The Spitzer data that we will obtain for WASP-17 are essential for us to fully understand exploit the Spitzer observations of exoplanets that will be obtained in the warm mission.

The structure, formation and fate of hot Jupiter exoplanets is governed by the properties of their atmospheres. There is an urgent need for for strong observational constraints to guide the development of model atmospheres for hot Jupiters. One of the most powerful techniques for probing hot Jupiter atmospheres is to observe the small variation in infrared flux through the orbital cycle for transiting hot Jupiters. These observations can be converted into a map of the temperature distribution around the planet. This gives us a direct measurement of the way heat is redistributed through the planet's atmosphere. The processes that redistribute heat from the day-side to the night-side in these tidally locked planets are very poorly understood. This limits our ability to interpret observations of hot Jupiters obtained with Spitzer and other instruments. Phase variations are small so they have only been succesfully observed in a handful of hot Jupiter systems. There are, as yet, no detections of the phase variation in any transiting hot-Jupiters with atmospheres hot enough to have a stratosphere, and only one (HD189733) for a cooler transiting hot Jupiter. We will observe the lightcurves of WASP-18 and WASP-19, to newly discovered ultra-short period planets (P<1day). These are key objects for understanding heat redistribution in hot Jupiters because the irradiation of their day-side is so extreme.

If both confirmed, it would turn out an interesting hot jupiter+brown dwarf system.

P.S

I've tried a simulation with Systemic Console using RV sets available. Surely additional data are required to confirm both or one of two objects, but a preliminary solution (with relatively low Chi and zero jitter) gives me a more eccentric orbit for brown dwarf (e=0.65) and a smaller orbital period for the hot jupiter (1.89 days rather 2.67 days). Hot planet's mass around 6 times that of Jupiter.

There is at least one case (HD 84117) where the observed velocity variability distribution appears to deviate significantly from a Gaussian distribution ... show no evidence for significant variability over the course of the 48n run, though no obvious periodocity, nor with an obviously Keplarian shape. (No other star observed on this run shows a similar variability trend, indicating that the variability seen is not a systematic effect of our measurement system. Adding additional AAPS data of similar quality taken in 2005 indicates that HD 84117 has shown excess velocity variability since 2005 over that expected from activity jitter alone (with an RMS of 4.7 m/s). The periodogram of HD 84117 shows essentially no power at periods of less than 40 d, though a complex, broad power distribution is seen at longer periods, i.e. longer than the time-span of the observations. We can therefore fit the data with no compelling single Keplarian. HD 84117 may either contain multiple planets, which will require intensive observation to disentangle, or may be a star with an unusual class of velocity variability. We can nonetheless say with confidence that it does not host a low-mass exoplanet in an orbit of less than ~30 d.

From that same paper, this time regarding HD 4308, which already is known to host a hot Neptune...

Finally, we note that the residuals to the Rocky Planet Search data alone (Fig. 4) are suggestive of a further periodicity in that data set at 30-40 d. To examine the possibility of there being a second planet present in this data, we have constructed the 2DKLS for the AAT and HARPS velocities with the Keplerian of Fig. 6 removed (see Fig. 7). The result is suggestive of power at period between 30-80 d. While potential planets at 32 d and 48 d periods can be fitted to this data, they do not do so with a significance that warrants a claim to have detected further planets in this system.